/ftp/cats/aliases/W/WHL



==========================================================================
J/MNRAS/436/275  Relaxation parameter of 2092 rich galaxy  clusters (Wen+, 2013)
The following files can be converted to FITS (extension .fit or fit.gz)
	table2.dat
==========================================================================
Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/MNRAS/436/275
==========================================================================

drwxr-xr-x 24 cats archive 4096 Feb 7 2022 [Up] drwxr-xr-x 4 cats archive 289 Jan 13 2023 [TAR file] -rw-r--r-- 1 cats archive 470 Dec 19 2022 .message -r--r--r-- 1 cats archive 4584 Dec 10 2014 ReadMe -rw-r--r-- 1 cats archive 871 Dec 10 2014 +footg5.gif -rw-r--r-- 1 cats archive 8391 Dec 10 2014 +footg8.gif -r--r--r-- 1 cats archive 192464 Oct 19 2014 table2.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : J/MNRAS/436/275 Relaxation parameter of 2092 rich galaxy clusters (Wen+, 2013) ================================================================================ Substructure and dynamical state of 2092 rich clusters of galaxies derived from photometric data. Wen Z.L., Han J.L. <Mon. Not. R. Astron. Soc., 436, 275-293 (2013)> =2013MNRAS.436..275W ================================================================================ ADC_Keywords: Clusters, galaxy ; Morphology Keywords: galaxies: clusters: general Abstract: Dynamical state of galaxy clusters is closely related to their observational properties in X-ray, optical and radio wavelengths. We develop a method to diagnose the substructure and dynamical state of galaxy clusters by using photometric data of Sloan Digital Sky Survey (SDSS). To trace mass distribution, the brightness distribution of member galaxies is smoothed by using a Gaussian kernel with a weight of their optical luminosities. After deriving the asymmetry, the ridge flatness and the normalized deviation of the smoothed optical map, we define a relaxation parameter, Gamma, to quantify dynamical state of clusters. This method is applied to a test sample of 98 clusters of 0.05<z< 0.42 collected from literature with known dynamical states and can recognize dynamical state for relaxed (Gamma>=0) and unrelaxed (Gamma<0) clusters with a success rate of 94 percent. We then calculate relaxation parameters of 2092 rich clusters previously identified from the SDSS, of which 28 percent clusters are dynamically relaxed with Gamma>=0. We find that the dominance and absolute magnitude of the brightest cluster galaxies closely correlate with dynamical states of clusters. The emission power of radio haloes is quantitatively related to cluster dynamical state, beside the known dependence on the X-ray luminosity. Description: We use the photometric data of the SDSS Data Release 8 (SDSS DR8, Aihara et al., 2011ApJS..193...29A) to discriminate luminous member galaxies and to estimate cluster richness and radius which will be used in the quantification of cluster dynamical state.